5 Aurigae is a triple star[7] system in the northern constellation of Auriga,[10] located about 195 light years away from the Sun based on parallax.[1] It is just visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.95.[2] The system is moving away from the Earth with a heliocentric radial velocity of +6 km/s,[6] having come within 62.4 light-years some 8.7 million years ago.[2]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 00m 18.33887s[1] |
| Declination | +39° 23′ 40.9241″[1] |
| Apparent magnitude (V) | 5.95[2] (6.02 + 9.50)[3] |
| Characteristics | |
| Spectral type | F5 V[4] |
| U−B color index | −0.03[5] |
| B−V color index | +0.42[5] |
| Astrometry | |
| Radial velocity (Rv) | +6.0±1.3[6] km/s |
| Proper motion (μ) | RA: −10.87[1] mas/yr Dec.: −1.08[1] mas/yr |
| Parallax (π) | 16.74 ± 0.71 mas[1] |
| Distance | 195 ± 8 ly (60 ± 3 pc) |
| Absolute magnitude (MV) | 2.07[2] |
| Orbit[7] | |
| Period (P) | 1,598.04±50.35 yr |
| Semi-major axis (a) | 5.379±0.388″ |
| Eccentricity (e) | 0.536±0.031 |
| Inclination (i) | 56.1±0.8° |
| Longitude of the node (Ω) | 155.4±0.7° |
| Periastron epoch (T) | 3,242.73±8.96 |
| Argument of periastron (ω) (secondary) | 333.4±4.5° |
| Details | |
| 5 Aur A | |
| Mass | 1.48[8] or 1.70[7] M☉ |
| Luminosity | 12.46[2] L☉ |
| Surface gravity (log g) | 4.14[8] cgs |
| Temperature | 6,603±225[8] K |
| Metallicity [Fe/H] | −0.02±0.07[9] dex |
| Age | 2.205[8] Gyr |
| 5 Aur B | |
| Mass | 0.82[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
This was initially discovered to be a binary star system by Otto Struve. The outer pair has an orbital period of 1,598 years with an eccentricity of 0.536.[7] The magnitude 6.02[3] primary, component A, is itself a binary system consisting of two stars of similar mass, roughly 1.5 times the mass of the Sun each, with an orbital period of 8.08 years.[11] It has a stellar classification of F5 V,[4] matching an F-type main-sequence star.
As of 2017, component B is a magnitude 9.50 star at an angular separation of 4.10″ from the primary along a position angle of 285°.[3]
References
edit- ^ a b c d e f van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
- ^ a b c d e Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b c Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. Vizier catalog entry
- ^ a b Abt, Helmut A. (2008). "Visual Multiples. IX. MK Spectral Types". The Astrophysical Journal Supplement Series. 176 (1): 216–217. Bibcode:2008ApJS..176..216A. doi:10.1086/525529.
- ^ a b Guetter, H. H. (1980). "UBV Photoelectric Photometry of 259 PZT Stars". Publications of the Astronomical Society of the Pacific. 92: 215. Bibcode:1980PASP...92..215G. doi:10.1086/130650.
- ^ a b Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ a b c d e Cvetkovic, Z.; Novakovic, B. (December 2006). "Orbits For Sixteen Binaries". Serbian Astronomical Journal. 173 (173): 73–82. Bibcode:2006SerAJ.173...73C. doi:10.2298/SAJ0673073C.
- ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ Gáspár, András; et al. (2016). "The Correlation between Metallicity and Debris Disk Mass". The Astrophysical Journal. 826 (2): 171. arXiv:1604.07403. Bibcode:2016ApJ...826..171G. doi:10.3847/0004-637X/826/2/171. S2CID 119241004.
- ^ a b "5 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-14.
- ^ Tokovinin, Andrei (2014). "From Binaries to Multiples. Ii. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 87. arXiv:1401.6827. Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87. S2CID 56066740.